6

The evolution of stars

• Stars recycle matter• No naked eye stars

have disappeared• Many stars have a

variable light output

The Glowing Eye of NGC 6751 in Aquilacourtesy NASA

Timescales

Hertzsprung-Russell diagram

Henry Norris Russell (1877 – 1957) Courtesy Margaret Olson, grand-daughter

Ejnar Hertzsprung (1873 – 1967)

Courtesy Kuhn & Koupelis fig 12.17

Stellar evolution

• Stars spend most of their life converting hydrogen to helium

• End game involves moving up and right

• Final state is a white dwarf

Fig 14.21 Courtesy Kuhn & Koupelis

Fusing hydrogen• Proton - proton chain reaction results:

4 protons + 2 electrons → helium + 6 γ + 2 ν

Hydrogen → Helium

• Loss of mass is about 0.7% (26.7 MeVper reaction)– using E = mc2, energy available for 1 kg

of hydrogen converted is 6.3×1014 J

••4 protons2 electrons

+ γ ν

He42 26.7 MeV

γν+

How long?

Fig. 14.5 courtesy Kuhn & Koupelis

Carbon cycle

• An alternative way of converting hydrogen to helium

• Faster than the proton-proton chain for stars more massive than 1.5 M

• Responsible for the short lives of massive stars– carbon 12 is converted by

fusion and β+ decay to nitrogen 15 before being recovered, along with helium 4 Fig 14.3 courtesy Kuhn & Koupelis

The beginning of the end

• Gravitational collapse

• Temperature increase

• Hydrogen fusing shell

• Expansion Fig 14.9 Courtesy Kuhn & Koupelis

A look ahead

• A → B becoming a red giant– inevitable for

stars 0.4 M to 4 M

• At B, the ‘helium flash’ for our sun

Fig 14.10 Courtesy Kuhn & Koupelis

Helium to carbon

• Essential for life• Short life of

beryllium makes this difficult

• Carbon 12 nuclear resonance helps

Figs 14.12 and 4.13 Courtesy Kuhn & Koupelis

Abundance of elements

• Formation abundance is dictated by conditions within the cores of dying stars

• Elements on Earth were formed in more than one star

• 108 K ≈ 104 eV– elements can be

created in particle accelerators

Source: http://www.cfa.ustc.edu.cn/course/CHAISSON/AT421/IMAGES/AACHDEI0.JPG

The final red-giant

phase• ~100 million

years for our Sun• Red-giants are

not intrinsically stable– escape velocity v2 = 2GM/r– ~ 40 km s-1

– substantial continuous emission of matter– pulses of emission create planetary nebulae

Fig 14.14 Courtesy Kuhn & Koupelis

NGC 2392 Eskimo nebula in Gemini ~ 5000 LY away

Courtesy HST: http://dayton.hq.nasa.gov/IMAGES/SMALL/GPN-2000-000882.jpg

NGC 6543 Cat’s eye nebula in Draco ~ 3000 LY distant

Courtesy HST: http://grin.hq.nasa.gov/IMAGES/SMALL/GPN-2000-000955.jpg

Courtesy HST: http://grin.hq.nasa.gov/IMAGES/SMALL/GPN-2000-001372.jpg

Stingray nebula in Ara ~ 18,000 LY distant

NGC 2346 Butterfly wing in Monoceros ~ 2000 LY distant

Courtesy HST: http://grin.hq.nasa.gov/IMAGES/SMALL/GPN-2000-000902.jpg

Courtesy HST: http://dayton.hq.nasa.gov/IMAGES/SMALL/GPN-2000-000964.jpg

M57 Ring nebula in Lyra ~ 2000 LY distant

Twin jet nebula in Ophiucus ~ 2100 LY distant

Courtesy HST: http://grin.hq.nasa.gov/IMAGES/SMALL/GPN-2000-000953.jpg

Courtesy HST: http://www.jpl.nasa.gov/images/wfpc/wfpc_110702_browse.jpg

NGC 6369 Little Ghost nebula in Ophiucus ~3000 LY distant

• White dwarves in M4

• ~ 12.5 billion years old

• Bottom right HST 8 day exposure of a region ~ 1 LY across– white dwarves

are circled in blue

White dwarvesCourtesy HST:

http://www.jpl.nasa.gov/images/wfpc/white_dwarf_stars_browse.jpg

• White dwarf reaches Chandrasekhar limit

• Standard candle M = -19

Figs 4.25 and 4.27 Courtesy Kuhn & Koupelis

Type Iasupernovae

Supergiants

• Massive stars create supergiants

• E.g. Betelgeuse

Fig 15.2 Courtesy Kuhn & Koupelis

Supergiant evolution

Fig 15.3 courtesy Kuhn & Koupelis

Evolution of a 15 solar mass star

Table 15.2 courtesy Kuhn & Koupelis

• Collapse of iron core• Protons → neutrons

+ neutrinos• Rebound wave

creates heavy elements + disperses ~ 5 M

• Crab nebula– ~ 6500 LY– supernova visible

by daylight in 1054

Type II supernova

Neutron stars

• The remnant core of a type II supernova explosion

• Between 1.4 and 3 M• Too small to be seen in a telescope

Courtesy Kuhn & Koupelis

Pulsars• Discovered by Jocelyn

Bell in 1967

← Image of the crab pulsar in X-rays by Chandra probe Source:

http://chandra.harvard.edu/photo/0052/0052_xray_lg.jpg

Fig. 15.13 Courtesy Kuhn & Koupelis

Black holes, again

• Black holes are the end game of supermassive stars

• Cores greater than about 3 M are too massive to form neutron stars– neutron degeneracy pressure cannot support the weight

• The core collapses to a black-hole– a 5 M black-hole has a Schwarzschild radius of 15 km

• this is not much smaller than a neutron star – Cygnus X-1, the first X-ray star discovered, behaves as a

binary with one component a black hole

Cygnus X-1 graphic, a binary with a massive B0 giant and a black hole

The end of

PX2512 lectures

6 The evolution of starsTimescalesHertzsprung-Russell diagramStellar evolutionFusing hydrogenHow long?Carbon cycleThe beginning of the endA look aheadHelium to carbonAbundance of elementsThe final red-giant phaseNGC 2392 Eskimo nebula in Gemini ~ 5000 LY awayNGC 6543 Cat’s eye nebula in Draco ~ 3000 LY distantStingray nebula in Ara ~ 18,000 LY distantNGC 2346 Butterfly wing in Monoceros ~ 2000 LY distantM57 Ring nebula in Lyra ~ 2000 LY distantTwin jet nebula in Ophiucus ~ 2100 LY distantNGC 6369 Little Ghost nebula in Ophiucus ~3000 LY distantWhite dwarvesType Ia supernovaeSupergiantsSupergiant evolutionEvolution of a 15 solar mass starType II supernovaNeutron starsPulsarsBlack holes, againThe end of PX2512 lectures